M3DIS - a grid of 3D radiation-hydrodynamics stellar atmosphere models for stellar surveys

• Verfasst von: Eitner, Philip [VerfasserIn]
• Verfasst von: Bergemann, Maria [VerfasserIn]
• Verfasst von: Hoppe, Richard [VerfasserIn]
• Verfasst von: Nordlund, Åke [VerfasserIn]
• Verfasst von: Plez, Bertrand [VerfasserIn]
• Verfasst von: Klevas, Jonas [VerfasserIn]
• Titel: M3DIS - a grid of 3D radiation-hydrodynamics stellar atmosphere models for stellar surveys
• Titelzusatz: I. Procedure, validation, and the sun
• Verf.angabe: Philipp Eitner, Maria Bergemann, Richard Hoppe, Åke Nordlund, Bertrand Plez, and Jonas Klevas
• E-Jahr: 2024
• Jahr: August 2024
• Umfang: 20 S.
• Illustrationen: Illustrationen
• Fussnoten: Online verfügbar: 2. August 2024 ; Gesehen am 30.06.2025
• Titel Quelle: Enthalten in: Astronomy and astrophysics
• Ort Quelle: Les Ulis : EDP Sciences, 1969
• Jahr Quelle: 2024
• Band/Heft Quelle: 688(2024) vom: Aug., Artikel-ID A52, Seite 1-20
• ISSN Quelle: 1432-0746
• DOI: doi:10.1051/0004-6361/202348448
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1929332823

Abstract

Context: Large-scale stellar surveys, such as SDSS-V, 4MOST, WEAVE, and PLATO, require accurate atmospheric models and synthetic spectra of stars for accurate analyses of fundamental stellar parameters and chemical abundances. Aims: The primary goal of our work is to develop a new approach to solve radiation-hydrodynamics (RHD) and generate model stellar spectra in a self-consistent and highly efficient framework. Methods: We build upon the Copenhagen legacy RHD code, the MULTI3D non-local thermodynamic equilibrium (NLTE) code, and the DISPATCH high-performance framework. The new approach allows us to calculate 3D RHD models of stellar atmospheres on timescales of a few thousand CPU hours and to perform subsequent spectrum synthesis in local thermodynamic equilibrium (LTE) or NLTE for the desired physical conditions within the parameter space of FGK-type stars. Results: We compare the 3D RHD solar model with other available models and validate its performance against solar observations, including the centre-to-limb variation of intensities and key solar diagnostic lines of H and Fe. We show that the performance of the new code allows to overcome the main bottleneck in 3D NLTE spectroscopy and enables calculations of multi-dimensional grids of synthetic stellar observables for comparison with modern astronomical observations.